1. ESO The other side of galaxy formation: radio line and continuum ‘Great Surveys’ Santa Fe November 2008 Chris Carilli NRAO

2. Cosmological deep fields: COSMOS o Definitive study of galaxy and SMBG evolution vs. environmnent o ACS: 600 orbits for 2deg 2 to I AB = 26 o VLA, Spitzer, 11-band SUBARU++, Galex, Chandra/XMM o Similar to SDSS in volume and resolution but at z > 1 o 2e6 galaxies from z~ 0 to 7

3. Star formation rate density vs. redshift ‘epoch of galaxy assembly’

4. Next level of detail: galaxy formation as function of M * ‘specific star formation rates’ = SFR/M * ‘Downsizing’ t H -1 ‘active star formation’ ‘red and dead’ Zheng+

5. Star formation history of Universe: dirty little secret UV correction factor ~ 5x Optical limitations  Dust obscuration: missing earliest, most active phases of galaxy formation  Only stars and star formation: not (cold) gas => missing the other half of the problem = ‘fuel for galaxy formation’

6. Radio astronomy: unveiling the cold, obscured universe Wilson et al. HST / OVRO CO  mm continuum: thermal emission from warm dust = star formation (see Yun)  (sub)mm lines: molecular gas, fine structure ISM cooling lines  (short) cm lines: low order molecular transitions, dynamics  cm continuum: synchrotron emission = star formation  (long) cm lines: HI 21cm (see Henning) 850um Class 0 protostar

7. COSMOS VLA deep16x  Full field at 1.4GHz  1.5” resolution  rms ~ 8 uJy/beam  4000 sources (10xHUDF) (mostly) star forming galaxies

8. 9 10 11 12 13 14 Log (FIR Luminosity) ULIRGs~Arp220 SFR ~ 100 M o /yr LIRGs~ M82 SFR~ 10 M o /yr AGN or Radio Surveys - Limits Milky Way SFR ~ 1 M o /yr 40uJy Submm gals: SFR > 10 3 M o yr -1

9. Pushing uJy radio studies to z>2: Stacking Cosmos BzK, LBG and LAE Median stacking of high-z ‘dropout’ samples in Cosmos field 30,000 BzK at z~1.3 to 2.5 8500 LBGs (U,B,V dropouts) at z~ 3, 4, 5 100 LAE in NB850 at z = 5.7 ‘normal’ star forming galaxy populations at high redshift Stacking analysis: ~ sub-uJy limits 4000A Ly-break BzK at z=1.7

10. 30,000 sBzK galaxies in Cosmos (>5x previous): Pannella+ star forming  nearIR selected: K AB ~ 23  M * ~ 10 10 to 10 11 M o  HST sizes ~ 1” ~ 9kpc Photo z z~1.3 to 2.5  Density ~ few x10 -4 Mpc -3 ~ 30x SMG  Forming ‘normal’ ellipticals, large spirals? 3.2” Daddi, McCracken + HST

11. 2e103e11 VLA stack 30,000 sBzK Pannella + = 8.8 +/- 0.1 uJy => ~ 96 M o yr -1 < 0.1x SMG Size ~ 1” SKA (sub-uJy) science before the SKA

12. S 1.4 increases with M * => SFR increases with stellar mass S 1.4 increases with B-z => dust extinction increases with SFR (or M * ) Stacking in bins of 4000 10 10 M o 3x10 11 M o

13. Dawn of Downsizing: SFR/M * vs. M * 5x t H -1 (z=1.8) z=0.3 1.4GHz SSFR z=1.5 z=2.1 UV SSFR  SSFR increases with z  SSFR constant with M *, unlike z ‘pre-downsizing’  z>1.5 sBzK well above the ‘red and dead’ galaxy line  Extinction increases with SFR, M *  UV dust correction needs to be differential wrt SFR, M *

14. Great Surveys: next gen radio deep fields Arcsec resolution is required to avoid confusion and detect ‘normal’ star forming galaxies at z > 1.5 All confusion limited (res>5”)

15. Early Universe Molecular Line Galaxies Submm galaxies: z ~ 1.5 to 4.5 SDSS J1335+3533 z=6.04  Gas mass (H 2 )~ 10 10 to 10 11 M o (~ 10 to 100x MW)  FIR > 10 13 L o => Star formation rates > 10 3 M o yr -1  Giant elliptical galaxy formation at high redshift? COSMOS J1000+0234 z=4.52 Most distant SMG QSO host galaxies: z ~ 1 to 6.4

16. SMBH ~ 1e9 M o Dust mass ~ 7e8 M o Gas mass ~ 2e10 M o CO size ~ 6 kpc Dynamical Mass ~ 4e10 M o Gas, Dust, Star Form, in host galaxy of J1148+5251 z=6.42 Only direct observations of host galaxy properties 1”

17.  FIR excess -- SED consistent with starburst: SFR ~ 3000 M o /yr  CO excitation ~ starburst nucleus: T kin ~ 100K, n H2 ~ 1e5 cm -3 Radio-FIR correlation 50K Elvis QSO SED Continuum SED and CO excitation: ISM physics at z=6.42 NGC253 MW

18. Building giant elliptical galaxies + SMBHs at t univ < 1Gyr z=6 QSO host stats (33 total) 10.5 8.1 6.5 Li, Hernquist, Roberston.. z=10  10 in dust: FIR > 1e13 L o  5 in CO: M gas > 1e10 M o  10 at 1.4 GHz continuum  2 in [CII] => SFR > 10 3 Mo yr -1 Rapid enrichment of metals, dust, molecules Rare, extreme mass objects: ~ 100 SDSS z~6 QSOs on entire sky

19. LFIR vs L’(CO) ~ SFR vs. total gas mass Integrated Schmidt-Kennicutt Law High-z sources = 10 -- 100 x M gas of Milky Way Index=1.5 Low z t dep ~3e8 yr Current sens ~ few x10 10 M o 1e3 M o /yr High z t dep ~1e7 yr Star formation efficiency = SFR per unit gas mass, increases with increasing SFR Gas depletion timescale = M gas /SFR decreases with SFR SFR Gas Mass

20. sBzK: not extreme starbursts, but massive gas reservoirs  6 of 6 sBzK detected in CO with Bure  Gas mass > 10 10 M o ~ submm galaxies, but  SFR < 10% submm gal  5 arcmin -2 (~50x submm galaxies) Daddi + 2008

21. Excitation = Milky Way (not starburst) FIR/L’CO = spiral (not starburst)  Extreme gas rich galaxies without extreme starbursts  Gas depletion timescales > 5 x10 8 yrs Starburst Dannerbauer + Daddi +

22. sBzK Low z ellipt ?? Current limitation: CO search requires optical pre-selection M gas >~ M *

23. Great Surveys: blind molecular line ‘piggy back’ surveys using 8GHz bandwidth EVLA: CO 1-0 at z = 1.4 to 1.9 (48 to 40 GHz)  FoV ~ 1 arcmin 2 => ~ 2 or 3 sBzK (M * > 10 10 M o )  rms (10hr, 300 km/s) = 50 uJy => L’(CO) = 1.9e9 K km/s pc 2  4  mass limit: M(H 2 ) = 3x10 10 M o (Galactic X factor) => Every ‘Q-band’ full synthesis will have ~ 1 sBzK CO detection ALMA: CO 2-1 at z = 1.45 to 1.7 (93 to 85 GHz)  FoV ~ 1 arcmin 2, but fractional BW (  z) ~ 1/2 EVLA  S 2-1 ~ 4xS 1-0 (in Jy) and rms (300 km/s) ~ 30uJy  Mass limit ~ 5x10 9 M o => Every ‘Band 3’ full synthesis will have ~ 3 sBzK CO detections

24. What is EVLA? First steps to the SKA By building on the existing infrastructure, multiply ten-fold the VLA’s observational capabilities, including 10x continuum sensitivity (1uJy), full frequency coverage (1 to 50 GHz), 80x BW (8GHz) Antenna retrofits now 50% completed. Early science Q1 2010, using new correlator. Full receiver complement completed 2012.

25. AOS Technical Building Array operations center What is ALMA? International collaboration to build & operate largest millimeter/submm array at 5000m in northern Chile -> order of magnitude, or more, improvement in all areas of (sub)mm astronomy, including resolution, sensitivity, and frequency coverage. Antenna commissioning in progress Antennas, receivers, correlator in production: best (sub)mm receivers and antennas ever! Site construction well under way: Observation Support Facility, Array Operations Site, antenna pads North American ALMA Science Center (C’Ville): support early science Q4 2010, full ops Q4 2012

26. ESO END